Author(s)

Ambrose C. Eze^1,2*, Sudum Esaenwi³, Abraham I. Chima⁴

¹Department of Physics and Geosciences, Faculty of Natural and Applied Sciences, Godfrey Okoye University, Enugu, Nigeria.
²Department of Physics and Astronomy, Faculty of Physical Sciences, University of Nigeria, Nsukka, Nigeria.
³NASRDA-Centre for Basic Space Science, Nsukka, Nigeria.
⁴Department of Industrial Physics, Enugu State University of Science and Technology, Enugu, Nigeria.

We present spectral analysis of Algol stellar flare data. The 2-day observation of Algol in our Galaxy was done by Suzaku Satellite. Algol binary system consists of two component stars that eclipse one another periodically. The stellar magnetic field activities and Roche Lobe overflow/mass transfer mechanisms during rapid rotation of the component stars generate an X-ray emission. The variation in brightness of the stellar flare from epoch to epoch provides useful information of stellar properties of the component stars. The atomic physics of the Kα line emission process in the vicinities of chromospherically active and X-ray flare stars, and binaries is well understood. The photo ionization/collisional excitation in the Algol’s corona produces 6.7 keV line emission. The accumulated spectra in X-ray Imaging Spectrometer (XIS) sensors fitted combined with bremsstrahlung model and Gaussian line show a strong fixed X-ray energy of 6.7 keV.

Flare Stars, Active Eclipsing Binary, Algol, Corona, Stellar Flare, X-Ray, Line Emission

Eze, A. , Esaenwi, S. and Chima, A. (2019) The 6.7 keV Line Emission from the Stellar Flare of Algol. Journal of High Energy Physics, Gravitation and Cosmology, 5, 1090-1097. doi: 10.4236/jhepgc.2019.54061.